We now review the results of HD simulations leveraging the metal tracing framework. In HR HD simulations, metals are a crucial tool to unveil and understand the kinematics of major physical processes, such as AGN feedback, SMBH feeding, and IGrM turbulence. While the detailed AGN self-regulation thermodynamics (cooling and heating cycle) is tackled in the companion [1]} review (see also the unification diagram in [2]}), here, we focus on the main IGrM cores kinematics features.
The SMBH/AGN at the center of each BGG or ETG is fed recurrently via chaotic cold accretion [3]}, i.e., the filamentary/cloudy condensation rain that is generated via nonlinear turbulent thermal instability in the IGrM hot halo ([4]}, [5]}; see also [6]}, [7]} for linear thermal instability simulations). Such frequent CCA clouds trigger the AGN feedback response by re-ejecting substantial amount of mass and energy via ultrafast outflows and relativistic jets [8]}, [9]}. At the macro scale of tens kpc, such entrained outflows/jets use their mechanical ram pressure to generate a diverse range of astrophysical phenomena (buoyant X-ray cavities, weak transonic shocks, turbulent eddies), which recurrently re-heat the IGrM halo and quench cooling flows/star formation throughout the several Gyr evolution [e.g. [10]}, [11]}, [12]}, [13]}, [14]}, [15]}, [16]}, [17]}, [18]}].
